The surface morphology and optical properties of Mercury resemble those of the moon in remarkable detail and record a very similar sequence of events. Chemical and mineralogical similarity of the outer layers of Mercury and the moon is implied; Mercury is probably a differentiated planet with a large iron-rich core. Differentiation is inferred to have occurred very early. No evidence of atmospheric modification of landforms has been found. Large-scale scarps and ridges unlike lunar or martian features may reflect a unique period of planetary compression near the end of heavy bombardment by small planetesimals.

The Mariner 10 television camieras imaged the planet Venus in the visible and near ultraviolet for a period of 8 days at resolutions ranging from 100 meters to 130 kilometers. Tle general pattern of the atmospheric circulation in the upper tropospheric/lower stratospheric region is displayed in the pictures. Atmospheric flow is symmetrical between north and south hemispheres. The equatorial motions are zonal (east-west) at approxiimnately 100 meters per second, consistent with the previously inferred 4-day retrograde rotation. Angular velocity increases with latitude. The subsolar region, and the region downwind from it, show evidence of large-scale convection that persists in spite of the main zonal motion. Dynamical interaction between the zonal motion and the relatively stationary region of convection is evidenced by bowlike waves.

Polarized and depolarized radar maps of the moon have been obtained at the Arecibo Ionospheric Observatory at a wavelength of 70 cm. These maps show strong positive anomalies, many of which are associated with young craters. These anomalies and the average diffuse component of radar echoes are attributed to the scattering behavior of surface and subsurface rocks. We have been able to approximately match the observed spatial and wavelength variation of the diffuse component, as well as the absolute value of its cross section, with theoretical calculations that use a Mie scattering description of the single scattering behavior of the rocks, and to employ the Surveyor spacecraft's determination of the size distribution of surface rocks. Furthermore, we have found that surface rocks appear capable of accounting for temperature anomalies (IR hot spots) which are associated with these craters.

Reflectivity and polarization laws for the powder sample and its spectrum are close to the mean for the lunar maria. Solid samples show a marked absorption feature at 1 micron. The low albedo appears to be due to a surface coating on dust grains rather than to volume absorption. The high-frequency electrical properties resemble those of a fine powder made from typical dense terrestrial rocks and are consistent with previous estimates from ground-based radar observations. The differential mass spectrum is almost constant from 100 micron particles down to 0.1 micron particles; most particles are smaller than 0.3 micron. Their shapes disclose a variety of processes of generation.

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